1. Physics 55 Friday, October 21, 2005 1.Doppler shift with application. 2.Conservation of angular momentum. 3.How star systems form, the nebular theory.

2. PRS Question I: Effect of Motion on Spectra? If light source is moving toward prism with speed v: 1.No change in absorption lines. 2.Absorption lines are blueshifted. 3.Absorption lines are redshifted 4.Some lines are redshifted, some are blueshifted

3. PRS Question II If thin cloud is moving away from prism with speed v: 1.No change in absorption lines. 2.Absorption lines are blueshifted. 3.Absorption lines are redshifted 4.Some lines are redshifted, some are blueshifted

4. PRS Question III If thin cloud 1 is moving toward the prism with speed v and thin cloud 2 is moving away from the prism with speed v 1.No change in absorption lines. 2.Absorption lines are blueshifted. 3.Absorption lines are redshifted 4.Some lines are redshifted, some are blueshifted.

5. Doppler Shifts Give Rotational Information

6. Doppler Shift Can Identify Binary Stars http://instruct1.cit.cornell.edu/courses/astro101/java/binary/binary.htm

7. Spectroscopic Binary Stars

8. Doppler Shift of Extrasolar Planets M S = mass Sun ~2 x 10 30 kg M J = mass Jupiter ~ 2 x 10 27 kg ~ 10 -3 M S L = Sun-Jupiter distance ~ 800 x 10 6 km Center of mass of Sun-Jupiter system ~ (M J /M S )L ~ d S ~ 742,000 km ~ 1.07 R S Speed of Sun in its small orbit: v = 2  d S / 12 y ~ 13 m/s, corresponds to incredibly small relative wavelength shifts  = v/c ~ 4 10 -8 Data from star 51 Pegasi (48 ly from Earth) implies presence of large planet with mass >~ 0.46 M Jupiter.

9. Need Right Geometry For Extrasolar Planets

10. Transit Method to Detect Extrasolar Planets Gives Size, Mass, Density so Kind From Wien’s law, we can deduce surface temperature T of remote star. From apparent brightness (intensity) I measured on Earth and distance to star d, we can deduce luminosity L of star: I = L / (4  d 2 ). From L and Stefan-Boltzmann, we can deduce radius of star R from equation: L = (4  R 2 ) (  T 4 ) From radius of star and decrease in relative brightness  f, we can deduce area and so radius r of occluding planet:  f = (  r 2 ) / (  R 2 ).

11. Extrasolar Planets

12. Overview of the Solar System

13. Other Parts of the Solar System: Asteroids, Kuiper Belt, Oort Cloud

14. Patterns of the Solar System

15. The Nebular Theory Orion Nebula Universal starting ingredients: 75% H 25% He

16. Gravity, Conservation of Energy, Momentum, Angular Momentum During Collapse of the Nebula Relatively short time to produce star and planets: ~10,000,000 y

17. Predictions of Nebular Theory 1.Existence of disks of around stars, most stars should therefore have planets. 2.Infrared thermal emission. 3.All objects rotate the same way (Doppler) 4.Two kinds of planets, small rocky terrestrial and large icy gaseous jovian planets. 5.Small rocky asteroids in ecliptic plane. 6.Small icy comets in ecliptic plane beyond jovian planets. 7.Small icy comets in all orientations far out into space. 8.Each solar system different in details because of random events.

18. Angular Momentum With Demos 1.Conservation of angular momentum holds for isolated systems. sum of all M x V x R before = sum of all M x V x R after 1.Application to speeds at aphelion/perihelion, apogee/perigee. 2.Demos: spinning chair, collapsing model of star.